[en] A part of the results obtained from the observation using K-9M-60 is presented. The excess in the energy region less than 0.1 KeV found in the energy spectra with the 0.5 μm PPL counter is described. The directional distributions of the L-band (0.15 to 0.3 KeV) and the LL band (0.06 to 0.15 KeV), and the energy spectra were obtained. The excess was seen in the energy spectrum of the LL band. The reason for this excess was considered and discussed. The noise spectrum of the counter is not a cause of the excess. As a result of discussion, it is suggested that the excess is due to other X-ray component with the energy less than L band. If this is true, the origin of the LL band X-ray may be a white dwarf or high temperature plasma. (Kato, T.)

[en] Three proportional counters with window film thickness of 0.96, 1.53 and 4.3 μm were used for the observation of North Polar Spur. The soft X-ray energy regions observed were the L-band (0.14 - 0.38 keV) and M-band (0.5 - 1.0 keV). The energy spectrum seems to be interpreted in terms of the X-ray emission from thin hot plasma. The present data indicate that the plasma consists of two components with temperature from 1 to 2 x 10⁶ deg K and of 5 x 10⁶ deg K. In the range from 0.4 to 1 keV, the emission lines of C-5, C-6, N-6, N-7, O-7, O-8, Fe-17 and Ne-9 contribute to the soft X-ray spectrum. The low temperature component is explained from heating by the shock wave generated by supernova explosion, and the high temperature component is explained as the emission from heated intercloud gas. (Yoshimori, M.)

[en] The purposes of the observation are to calibrate the instrument with X-ray from Crab Nebula, to search for X ray from MONOCEROS supernova, to investigate the structure and the energy spectrum in the strong X-ray regions in Gemini and Eridanus, and to search for X ray from Orion region. The soft X ray detectors employed in the present observation were eight membrane proportional counters and a multi-wire proportional counter. To improve the energy resolution, 1 μm, 1.5 μm and 3 μm thick polypropylene filters and 120 μg/cm² thick boron filter were used. The effective area of one proportional counter was 134 cm² and soft X-ray between 0.4 and 2 keV was detected. The sandhawk rocket was launched on Nov. 9, 1974, and the aspect control was made. The expected observation was made. (J.P.N.)

[en] The sky mapping of especially the isotropic component of soft X-ray of galactic origin has been made to investigate the origin of soft X-ray. It is well known that the spatial distribution of the isotropic component of galactic soft X-ray depends largely on their energy, but proportional counters have not enough energy resolution to resolution to resolve the soft X-ray energy. To improve the energy resolution, filters have been used. In this observation, the K-absorption edges of boron (0.18 keV) and polypropylene (0.28 keV) were utilized as the filters to resolve X-ray energy. The effective area of the proportional counter was 600 cm², and the collimating field of view was 3 deg x 10 deg. The K-9M-50 rocket was launched on Jan. 23, 1975. The data on galactic soft X-ray between 0.1 and 2 keV are being analyzed, but the energy spectrum measured is presented. (J.P.N.)

[en] Recent reports have indicated that depiction of the thoracic duct is possible without administration of a contrast agent using fast advanced spin echo (FASE), electrocardiogram (ECG)-triggered, half-Fourier fast spin echo (FSE), by depicting blood vessels. In this study, we attempted to depict the thoracic duct using FASE, which is generally used for MR-hydrography. By varying effective echo time (effective TE), the contrast-to-noise ratios (CNR) for saline and baby oil were measured with and without fat suppression. Without fat suppression, the effective TE of 500 msec yielded the highest CNR. With fat suppression, the effective TE of 250 msec provided the highest CNR. Next, examinations of the thoracic duct were performed in volunteers in order to obtain the highest CNR. Results indicated that the best depiction of the thoracic duct was obtained using the effective TE of 500 msec in 3D-FASE without fat suppression. Thoracic duct imaging using heavily T₂-weighted parameters allows better control of signal intensities of background and surrounding tissues than can be obtained with fat suppression. Furthermore, the heavily T₂-weighted parameter only depicts the long T₂ components of the thoracic duct. (author)